Abstract: I explain my investigation into how supernovae power turbulence in the ISMs of starburst regions, and the implications for magnetic fields and cosmic rays. In weaker starbursts, supernovae blast open a hot (~40 MK) phase that escapes as a superwind. I calculate that supernovae can drive Mach ~ 1 turbulence in the hot wind. In the densest starbursts, like Arp 220, the volume is instead filled by cold molecular gas. Supernovae alone can drive turbulence in this gas to ~20 - 30 km/s, despite strong radiative losses. I predict magnetic field strengths of 70 microGauss in the Galactic Center starburst, 200 microGauss in NGC 253 and M82, and 2 milliGauss in Arp 220's nuclei. I show how supernova driving of turbulence naturally results in equipartition between several ISM phases in starbursts. I also discuss why CR diffusion may be very slow in these regions. Instead, turbulent mixing by the ISM may transport CRs, a very different process.

Abstract: The transport of high-energy charged particles in the turbulent plasmas of the heliosphere and the interstellar medium is one of the key problems in cosmic ray physics. Understanding the transport process by means of analytical calculations by the extreme complexity of the non-linear wave-particle interaction charged particles undergo.
In the past many attempt have been undertaken to perform numerical simulations of the transport of charged particles. Most of these attempt have been using artificial turbulence. I will show now our recent model combining incompressible MHD simulations with test particle transport.
I will especially focus on the problems associated with deciphering the pitch-angle diffusion from the tracks of test particles in a turbulent plasma.